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Fig. 11.


Comparison of the metallicity distribution as a function of H I column density for quasar and GRB absorbers with C I or H2 detections. Blue filled circles again denote the GRBs with C I detected in absorption (empty blue circles show the GRBs with C I detected below the completeness limit). Overplotted are the quasar absorbers with H2 detections from the VLT/UVES sample (dark red squares), quasar absorbers selected for the presence of the 2175 Å dust extinction feature (green diamonds) and quasar absorbers selected for the presence of C I absorption (yellow squares). Only systems with Wr(λ 1560)> 0.2 Å from each of the C I samples are shown. The dashed lines mark constant values of logN(H I)/cm−2 + [X/H] as indicated at each line.

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